Beyond BAO Eiichiro Komatsu (Univ. of Texas at Austin) MPE Seminar, - PowerPoint PPT Presentation

Beyond BAO Eiichiro Komatsu (Univ. of Texas at Austin) MPE Seminar, August 7, 2008 1

Papers To Talk About • Donghui Jeong & EK, ApJ, 651, 619 (2006) • Donghui Jeong & EK, arXiv:0805.2632 • Masatoshi Shoji, Donghui Jeong & EK, arXiv:0805.4238 • Jeong, Sefusatti & Komatsu (in preparation) 2

Why BAO? In 5 Minutes • We can measure: • Angular Diameter Distances, D A (z) • Hubble Expansion Rates, H(z) • D A (z) & H(z). These are fundamental quantities to measure in cosmology! 3

Transverse=D A (z); Radial=H(z) SDSS Data Linear Theory Two-point correlation c Δ z/(1+z) function measured = d s (z BAO ) H(z) from the SDSS Luminous Red Galaxies (Okumura et al. 2007) (1+z)d s (z BAO ) 4 θ = d s (z BAO )/ D A (z)

BAO as a Standard Ruler Okumura et al. (2007) Position Space Fourier Space Percival et al. (2006) (1+z)d BAO • The existence of a localized clustering scale in the 2-point function yields oscillations in Fourier space. 5

D V (z) = {(1+z) 2 D A2 (z)[cz/H(z)]} 1/3 Once spherically averaged, D A (z) and H(z) are mixed. A combination distance, D V (z) , has been constrained. (1+z)d s ( t BAO )/D V (z) 2dFGRS and SDSS main samples SDSS LRG samples Ω m =1, Ω Λ =1 Ω m =0.3, Ω Λ =0 Ω m =0.25, Ω Λ =0.75 6 Redshift, z Percival et al. (2007)

H(z) also determined recently! • SDSS DR6 data are now good enough to constrain H(z) from the 2-dimension correlation function without spherical averaging . • Excellent agreement with Λ CDM model. 7 Gaztanaga, Cabre & Hui (2008)

Why Go Beyond BAO? • BAOs capture only a fraction of the information contained in the galaxy power spectrum! • BAOs use the sound horizon size at z~1020 as the standard ruler. • However, there are other standard rulers: • Horizon size at the matter-radiation equality epoch (z~3200) • Silk damping scale 8

Eisenstein & Hu (1998) BAO 9

...and, these are all well known • Cosmologists have been measuring k eq over the last three decades. • This was usually called the “Shape Parameter,” denoted as Γ . • Γ is proportional to k eq /h, and: • The effect of the Silk damping is contained in the constant of proportionality. • Easier to measure than BAOs: the signal is much stronger. 10

WMAP & Standard Ruler • With WMAP 5-year data only, the scales of the standard rulers have been determined accurately (Komatsu et al. 2008). Even when w ≠ -1, Ω k ≠ 0, • d s (z BAO ) = 153.4 +1.9-2.0 Mpc (z BAO =1019.8 ± 1.5) 1.3% • k eq =(0.975 +0.044-0.045 )x10 -2 Mpc -1 (z eq =3198 +145-146 ) 4.6% • k silk =(8.83 ± 0.20)x10 -2 Mpc -1 2.3% With Planck, they will be determined to higher precision. 11

Shoji, Jeong & Komatsu (2008) BAO vs Full Modeling 1.10 BAO only • Full modeling improves upon 1.05 the determinations of D A & H H/H ref bestfit=1.000 Full by more than a factor of two. 1.00 • On the D A -H plane, the size of the ellipse shrinks by more 0.95 than a factor of four. 12 For HETDEX 0.90 0.90 0.95 1.00 1.05 1.10 D A /D A,ref bestfit=1.000

Shoji, Jeong & Komatsu (2008) For the analysis of HETDEX • BAO only • D A : 2.1%, H: 2.6% • Correlation coefficient: 0.43 • Full Modeling • D A : 0.96%, H: 0.80% • Correlation coefficient: -0.79 13

HETDEX ？ • www.hetdex.org 14

Effective Use of Resources • Using the full information is equivalent to having four times as much volume as you would have with the BAO-only analysis. • Save the integration time by a factor of four! 15

Still, BAO. • If what I am saying is correct, why would people talk only about the BAOs these days, and tend to ignore the full information? • NON-LINEARITY 16

Non-linear Effects • Three non-linearities 1. Non-linear matter clustering Real Data 2. Non-linear galaxy bias Linear Theory 3. Non-linear peculiar velocity The effects of k eq and k silk can be affected by these non-linear effects much more strongly OK for BAO? than the effects of BAOs. 17

Seo, Siegel, Eisenstein & White (2008) According to Dan Eisenstein: • The phases of BAOs are not affected by the non-linear evolution very much. • The effects are correctable. • z=0.3: 0.54% • z=1.5: 0.25% 18

Takada, Komatsu & Futamase (2006) Why Full Information? Reason II • Not only do we improve upon the determinations of D A & H, but also: • We can constrain inflationary models, and • We can measure the neutrino masses and the number of massive neutrino species. • Therefore, just using the BAOs is such a waste of information! 19

Toward Understanding Non-linearities • Three non-linearities 1. Non-linear matter clustering Real Data 2. Non-linear galaxy bias Linear Theory 3. Non-linear peculiar velocity Solid theoretical framework is necessary for avoiding any OK for BAO? empirical, calibration factors 20

Toward Understanding Non-linearities • Solid framework: Perturbation Theory (PT) • Validity of the cosmological linear perturbation theory has been verified observationally (Remember WMAP!) • So, we just go beyond the linear theory, and calculate higher order terms in perturbations. • 3rd-order perturbation theory (3PT) 21

Is 3PT New? • No. It is more than 25 years old. • Active investigations in 1990’s • Most popular in European and Asian countries, but was not very popular in USA for some reason • 3PT has never been applied to the real data so far. Why? • Non-linearity is too strong to model by PT at z~0 22

Why Perturbation Theory Now? • The time has changed. • High-redshift (z>1) galaxy redshift surveys are now possible. • And now, such surveys are needed for Dark Energy studies • Non-linearities are weaker at z>1, making it possible to use the cosmological perturbation theory! 23

Just Three Equations to Solve • Consider large scales, where the baryon pressure is negligible, i.e., the scales larger than the Jeans scale • Ignore the shell-crossing, i.e., the velocity field of particles has zero curl: rot V =0. • Equations to solve are: 24

Fourier Transform... ˙ δ ( k , τ ) + θ ( k , τ ) d 3 k 1 d 3 k 2 δ D ( k 1 + k 2 − k ) k · k 1 � � = δ ( k 2 , τ ) θ ( k 1 , τ ) , − k 2 (2 π ) 3 1 a 2 θ ( k , τ ) + ˙ a θ ( k , τ ) + 3˙ a ˙ 2 a 2 Ω m ( τ ) δ ( k , τ ) d 3 k 1 d 3 k 2 δ D ( k 1 + k 2 − k ) k 2 ( k 1 · k 2 ) � � = θ ( k 1 , τ ) θ ( k 2 , τ ) , − 2 k 2 1 k 2 (2 π ) 3 2 • Here, is the velocity divergence. 25

Taylor-expand in δ 1 • δ 1 is the linear perturbation n ∞ (2 π ) 3 · · · d 3 q n − 1 d 3 q 1 � � � � a n ( τ ) d 3 q n δ D ( δ ( k , τ ) = q i − k ) F n ( q 1 , q 2 , · · · , q n ) δ 1 ( q 1 ) · · · δ 1 ( q n ) , (2 π ) 3 n =1 i =1 n ∞ (2 π ) 3 · · · d 3 q n − 1 d 3 q 1 � � � � a ( τ ) a n − 1 ( τ ) d 3 q n δ D ( θ ( k , τ ) = − ˙ q i − k ) G n ( q 1 , q 2 , · · · , q n ) δ 1 ( q 1 ) · · · δ 1 ( q n ) (2 π ) 3 n =1 i =1 26

Keep terms up to 3rd order • δ = δ 1 + δ 2 + δ 3 , where δ 2 =O( δ 12 ), δ 3 =O( δ 13 ). • Power spectrum, P(k)= P L (k) + P 22 (k) +2 P 13 (k) , may be written, order-by-order, as Odd powers in δ 1 vanish (Gaussianity) P L P 13 P 22 P 13 27

Vishniac (1983); Fry (1984); Goroff et al. (1986); Suto&Sasaki (1991); Makino et al. (1992); Jain&Bertschinger (1994); Scoccimarro&Frieman (1996) P(k): 3rd-order Solution d 3 q � � 2 � F ( s ) P 22 ( k ) = 2 (2 π ) 3 P L ( q ) P L ( | k − q | ) 2 ( q , k − q ) , � ∞ 2 π k 2 dq 2 P 13 ( k ) = 252 P L ( k ) (2 π ) 3 P L ( q ) 0 � 100 q 2 k 2 − 158 + 12 k 2 q 2 − 42 q 4 × k 4 � k + q � � 3 k 5 q 3 ( q 2 − k 2 ) 3 (2 k 2 + 7 q 2 ) ln + , | k − q | • F 2(s) is a known mathematical function (Goroff et al. 1986) 28

Jeong & Komatsu (2006) 3PT vs N-body Simulations 29

Jeong & Komatsu (2006) BAO: Matter Non-linearity Simulation 3rd-order PT Linear theory 30

What About Galaxies? • We measure the galaxy power spectrum. • Who cares about the matter power spectrum? • How can we use 3PT for galaxies? 31

Local Bias Assumption • The distribution of galaxies is not the same as the distribution of matter fluctuations • Usually, this fact is modeled by the so-called “linear bias,” meaning P g (k)=b 12 P(k), where b 1 a scale-independent (but time-dependent) factor. • How do we extend this to the non-linear form? We have to assume something about the galaxy formation • Assumption: galaxy formation is a local process, at least on the scales that cosmologists care about. 32

Gaztanaga & Fry (1993); McDonald (2006) Taylor-expand δ g in δ δ g (x) = c 1 δ (x) + c 2 δ 2 (x) + c 3 δ 3 (x) + O( δ 4 ) + ε (x) Here, δ is the non-linear matter perturbation, ε is stocastic “noise,” uncorrelated with δ , i.e., < δ (x) ε (x)>=0. • Both sides of this equation are evaluated at the same spatial location, x, hence the term “local.” • We know that the local assumption breaks down at some small scales. That’s where we must stop using PT. 33